We notice that \(\Lambda _i\)  depends directly on the stiffness of the EoS through the compactness \(\beta \)  and indirectly through the speed of sound which appears in Eq. (REF ). The dependence of \(\Lambda _i\)  on the behavior of \(y(R)\)  can lead to useful estimations or constraints on the tidal deformability itself. To be more specific, the applied EoS affects also the behavior of \(\Lambda \)  regarding the neutron star's mass \(M\)  and radius \(R\)  . In our study we use the secondary very massive component of GW190814 system (see Ref. [1]}) to examine the tidal deformability and the behavior of dense nuclear matter in the extreme scenario of such a massive neutron star.
